Bouwens et al. 2008, ApJ, 686, 230 Bouwens et al. 2010, Nature, Submitted

1. 1. Introduction 4. Development & Test Plan 3. Scientific Targets 2. Specifications of the FPC-S * Related Papers Near-Infrared Instrument for SPICA : FPC–S (Focal Plane Camera – Science) Dae-Hee Lee1, Woong-Seob Jeong1, Toshio Matsumoto2,3, Hyung Mok Lee2, Myungshin Im2, Bon-Chul Koo2, Masateru Ishiguro2, Jonghak Woo2, Myung Gyoon Lee2, Soojong Pak4, Sung-Joon Park1, Bongkon Moon1, Chang Hee Ree1, Youngsik Park1, Uk-Won Nam1, Jeonghyun Pyo1, Keon Hee Kim5, Kohji Tsumura3, Wonyong Han1, and Korean Consortium for FPC-S1,2,3,4,5,6 1 Korea Astronomy and Space Science Institute, Korea, 2 Seoul National University, Korea, 3 Institute of Space and Astronautical Science, JAXA, Japan, 4 Kyung Hee University, Korea, 5 Korea Basic Science Institute, Korea, 6 National Astronomical Observatory of Japan, Japan • 3.1 Legacy Programs • Near-Infrared Spectroscopic Survey with FPC for Cosmic IR Background and Extragalactic Sciences (NIRSS) • Wide Field Spectroscopic Survey with LVF (R~20) • Primary Science: Cosmic Infrared Background Radiation: Fluctuation and Spectrum • Measurement of the spectrum of the sky to examine the nature of the excess background emission • Detection of the fluctuation of the sky brightness caused by Pop.III stars. • Secondary Sciences: Lyman Break Galaxies up to redshift 10, Emission Line Galaxies • Understanding of high redshift star formation history of the Universe and the reionization • Direct detection of Lyman break galaxies (z~5 – 10) • Based upon the previous collaboration in IR projects between Korea and Japan, Korea propose the near-infrared instrument for SPICA, FPC (Focal Plane Camera). • The FPC consists of two parts; one is FPC-S (fine Guider) and the other is FPC-S (Science). • The primary function of the FPC-S is the back-up system of FPC-G and it also performs scientific observations. • It has a capability of wide-band imaging as well as imaging spectroscopy using LVF (Linear Variable Filter). • Korea Astronomy & Space Science Institute (KASI) will lead the development , assembly and test of the FPC-S. Korea’s involvement in IR Projects SPICA FPC AKARI DR Pipeline Science Collaborations Soothed image of infrared excess emission after subtracting the contributions from Zodiacal light and point sources of Monitor field observed by AKARI. Angular diameter is 10 arcmin and wavelength band is 2.4, 3.2 and 4.1m from left to right (Matsumoto et al. 2010) Space IR MIRIS Compact Space IR Camera CIBER Near-IR Camera Ground IR Excess power spectrum at 2.4m observed with AKARI PSICS IR Cryogenic System IGRINS Ground Near-IR Spectrometer KASINICS Ground Near-IR Camera 2004 2006 2008 2010 2012 2014 • Parallel Imaging Survey for Extragalactic Sciences • Parallel observations with other instruments • Wider areal and spectral coverage • 180 deg2 (5-year lifetime, 4 filters) UV luminosity function at z~4, 7, 8 and 10 (Bouwens et al. 2010). Two vertical lines show the sensitivity limit at rest frame for z~6 and 10, respectively. LBG samples from HST observation (Bouwens et al. 2008). The red square shows the pixel scale of FPC-S. • 3.2 Target of Opportunities: Comet Observations, Gamma Ray Bursts … Specifications Optical & Structural Design Bouwens et al. 2008, ApJ, 686, 230 Bouwens et al. 2010, Nature, Submitted Matsumoto et al. 2010, ApJ, Submitted